Current sheets in the solar corona

Details Current sheets in the solar corona Current sheets in the solar corona

Mar 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...326..418s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 326, March 1, 1988, p. 418-424.

Astronomy and Astrophysics

Astrophysics

52

Current Sheets, Magnetohydrodynamic Stability, Plasma Heating, Solar Corona, Magnetic Field Reconnection, Ohmic Dissipation, Resistance Heating

Scientific paper

Coronal magnetic fields are twisted up by motion of their footpoints in the photosphere. When the twist exceeds a critial amount, kink-ballooning instabilities occur. The authors study these instabilities numerically, in long, thin, axially bounded magnetic fields. Nonlinearly, the three-dimensional kinking motion compresses magnetic flux, forming a current sheet. Magnetic energy can be dissipated at a rate orders of magnitude greater than without the current sheets. The energy of footpoint motion can then go into coronal heating, via Ohmic dissipation in the current sheets.

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